Researchers have developed an analytical framework to quantify the impact of stray light on the sensitivity of ground-based gravitational wave interferometers. This model directly translates detector sensitivity requirements into design specifications for the core optics region, a crucial step in mitigating a noise source that can compromise the detection of extremely faint gravitational signals. The work addresses various scattering regimes and extends the analysis to collections of planar baffles, as well as deterministic ghost beams intercepted by beam dumps.

The new framework provides conservative estimates for early design phases, even before a complete optical layout of the detector is available. This capability is fundamental for planning the next generation of gravitational wave observatories, such as Cosmic Explorer, where noise reduction is paramount for achieving unprecedented sensitivities. The authors applied their methodology to Cosmic Explorer, demonstrating how these estimates can guide design requirements for these cutting-edge instruments.

The resulting expressions offer a compact set of tools for stray light budgeting and early design studies. This will facilitate the optimization of optical components and detector layouts, ensuring that stray light noise remains below critical thresholds. The ability to predict and mitigate this type of noise from the initial design stages is essential for maximizing the discovery potential of future gravitational wave observatories, enabling the exploration of even more distant and subtle astrophysical phenomena.